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SUMMARY:Cosmic-Ray Transport in Interstellar Medium
DTSTART;VALUE=DATE-TIME:20260716T012000Z
DTEND;VALUE=DATE-TIME:20260716T015000Z
DTSTAMP;VALUE=DATE-TIME:20260722T050748Z
UID:indico-contribution-2502-8972@indico.icrr.u-tokyo.ac.jp
DESCRIPTION:Speakers: Ryohei Inamoto ()\nCosmic rays are a key probe of hi
 gh-energy astrophysical phenomena across a broad wavelength range\, from r
 adio to gamma rays\, and may also play an important role in regulating gal
 axy evolution. However\, how cosmic rays are transported in and around gal
 axies\, and how they feed back on gas and magnetic fields\, remain poorly 
 understood. To investigate these two aspects of cosmic rays in a unified f
 ramework\, we are developing a numerical code that treats cosmic-ray trans
 port and dynamical feedback self-consistently. Recent improvements to the 
 code have enabled us to stably follow the long-term evolution of star-form
 ation-driven winds interacting with cold gas clouds under more realistic p
 hysical conditions. In this talk\, I will present an overview of the code 
 and discuss numerical results on how cosmic-ray transport affects the dyna
 mical evolution of cold gas clouds in the galactic halo.\n\nhttps://indico
 .icrr.u-tokyo.ac.jp/event/1254/contributions/8972/
LOCATION:Kashiwa Large Seminar Room 601 (Kashiwa)
URL:https://indico.icrr.u-tokyo.ac.jp/event/1254/contributions/8972/
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SUMMARY:Cosmic-Ray Acceleration on supernova remnant shocks
DTSTART;VALUE=DATE-TIME:20260716T005000Z
DTEND;VALUE=DATE-TIME:20260716T012000Z
DTSTAMP;VALUE=DATE-TIME:20260722T050748Z
UID:indico-contribution-2502-8971@indico.icrr.u-tokyo.ac.jp
DESCRIPTION:Speakers: Ryosuke Kobashi ()\nSupernova remnants (SNRs) have b
 een considered as the sources of the bulk of Galactic cosmic-ray (CR). Rec
 ently some evidences of extended gamma-ray emission are reported by e.g. L
 HAASO and H.E.S.S. and this emission infers the existence of particles esc
 aping from accelerating region of SNRs. \nIn this work\, we solve one-dime
 nsional diffusion-convection equation coupled with analytical solutions fo
 r shock dynamics\, to obtain the time evolution of phase-space distributio
 n function of CR. As a result\, the time evolution of CR acceleration stil
 l increases even after the age of 10kyrs in our models\, and this behavior
  is largely affected by environment of SNRs.\n\nhttps://indico.icrr.u-toky
 o.ac.jp/event/1254/contributions/8971/
LOCATION:Kashiwa Large Seminar Room 601 (Kashiwa)
URL:https://indico.icrr.u-tokyo.ac.jp/event/1254/contributions/8971/
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